@Article{SousaCoelAraú:2020:GrWaSG,
               author = "Sousa, Manoel Felipe and Coelho, Jaziel Gourlart and Ara{\'u}jo, 
                         Jos{\'e} Carlos Neves de",
          affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and 
                         {Universidade Tecnologica Federal do Paran{\'a} (UTFPR)} and 
                         {Instituto Nacional de Pesquisas Espaciais (INPE)}",
                title = "Gravitational waves from SGRs and AXPs as fast-spinning white 
                         dwarfs",
              journal = "Monthly Notices of the Royal Astronomical Society",
                 year = "2020",
               volume = "498",
               number = "3",
                pages = "4426--4432",
                month = "Nov.",
             keywords = "gravitational waves – stars: magnetic field – white dwarfs.",
             abstract = "In our previous article we have explored the continuous 
                         gravitational waves (GWs) emitted from rotating magnetized white 
                         dwarfs (WDs) and their detectability by the planned GW detectors 
                         such as Laser Interferometer Space Antenna (LISA), Decihertz 
                         Interferometer Gravitational wave Observatory (DECIGO), and Big 
                         Bang Observer (BBO). Here, GWs emission due to magnetic 
                         deformation mechanism is applied for soft gamma repeaters (SGRs) 
                         and anomalous X-ray pulsars (AXPs), described as fast-spinning and 
                         magnetized WDs. Such emission is caused by the asymmetry around 
                         the rotation axis of the star generated by its own intense 
                         magnetic field. Thus, for the first time in the literature, the GW 
                         counterparts for SGRs/AXPs are described as WD pulsars. We find 
                         that some SGRs/AXPs can be observed by the space detectors BBO and 
                         DECIGO. In particular, 1E 1547.0\−5408 and SGR 
                         1806\−20 could be detected in 1 yr of observation, whereas 
                         SGR 1900+14, CXOU J171405.7\−381031, Swift 
                         J1834.9\−0846, SGR 1627\−41, PSR J1622\−4950, 
                         SGR J1745\−2900, and SGR 1935+2154 could be observed with a 
                         5-yr observation time. The sources XTE J1810\−197, SGR 
                         0501+4516, and 1E 1048.1\−5937 could also be seen by BBO 
                         and DECIGO if these objects have MWD 1.3 M and MWD 1.2 M, 
                         respectively. We also found that SGRs/AXPs as highly magnetized 
                         neutron stars are far below the sensitivity curves of BBO and 
                         DECIGO. This result indicates that a possible detection of 
                         continuous GWs originated from these objects would corroborate the 
                         WD pulsar model.",
                  doi = "10.1093/mnras/staa2683",
                  url = "http://dx.doi.org/10.1093/mnras/staa2683",
                 issn = "0035-8711 and 1365-2966",
             language = "en",
           targetfile = "sousa_gravitational2.pdf",
        urlaccessdate = "09 maio 2024"
}